Hostname: page-component-586b7cd67f-tf8b9 Total loading time: 0 Render date: 2024-11-24T23:21:43.603Z Has data issue: false hasContentIssue false

Automated Extraction of DIBs from Cool Star Spectra

Published online by Cambridge University Press:  21 February 2014

H.-Ch. Chen
Affiliation:
GEPI Observatoire de Paris, CNRS, Université Paris-Diderot, Place Jules Janssen, F-92195 Meudon Cedex, France email: [email protected]
R. Lallement
Affiliation:
GEPI Observatoire de Paris, CNRS, Université Paris-Diderot, Place Jules Janssen, F-92195 Meudon Cedex, France email: [email protected]
L. Puspitarini
Affiliation:
GEPI Observatoire de Paris, CNRS, Université Paris-Diderot, Place Jules Janssen, F-92195 Meudon Cedex, France email: [email protected]
P. Bonifacio
Affiliation:
GEPI Observatoire de Paris, CNRS, Université Paris-Diderot, Place Jules Janssen, F-92195 Meudon Cedex, France email: [email protected]
C. Babusiaux
Affiliation:
GEPI Observatoire de Paris, CNRS, Université Paris-Diderot, Place Jules Janssen, F-92195 Meudon Cedex, France email: [email protected]
V. Hill
Affiliation:
Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d'Azur, Laboratoire Cassiopée, B.P. 4229, 06304 Nice Cedex 4, France
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have developed a method allowing to extract DIBs from cool star spectra, based on combinations of stellar synthetic, telluric transmission (when necessary), and DIB profile models. It is applicable when the star temperature, surface gravity and metallicity have been previously estimated. Such a method aims at extracting extensive data from stellar spectroscopic surveys such as the Gaia-ESO Survey in progress at the VLT. The method has been applied to several strong DIBs detected towards stars from various programs and located at various distances from the solar neighborhood to the Galactic Bulge. Here we illustrate the extraction of the 8620 Å DIB, and compare its strength to the one of the 6284 Å band, both for nearby and bulge stars.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2014 

References

Chen, H.-C., Lallement, R., Babusiaux, C., et al. 2013, A&A, 550, A62Google Scholar
Clough, S. A., Shephard, M. W., Mlawer, E. J., et al. 2005, Journal of Quantitative Spectroscopy and Radiative Transfer, 91, 233Google Scholar
Kurucz, R. L. 2005, Memorie della Societa Astronomica Italiana Supplementi, 8, 14Google Scholar
Munari, U., Tomasella, L., Fiorucci, M., et al. 2008, A&A, 488, 969Google Scholar
Puspitarini, L., Lallement, R., & Chen, H.-C. 2013, A&A, 555, A25Google Scholar
Raimond, S., Lallement, R., Vergely, J. L., Babusiaux, C., & Eyer, L. 2012, A&A, 544, A136Google Scholar
Rothman, L. S., Gordon, I. E., Barbe, A., et al. 2009, Journal of Quantitative Spectroscopy and Radiative Transfer, 110, 533Google Scholar
Sbordone, L., Bonifacio, P., Castelli, F., & Kurucz, R. L. 2004, Memorie della Societa Astronomica Italiana Supplementi, 5, 93Google Scholar
Sbordone, L. 2005, Memorie della Societa Astronomica Italiana Supplementi, 8, 61Google Scholar
Vergely, J.-L., Valette, B., Lallement, R., & Raimond, S. 2010, A&A, 518, A31Google Scholar
Vos, D. A. I., Cox, N. L. J., Kaper, L., Spaans, M., & Ehrenfreund, P. 2011, A&A, 533, A129Google Scholar